In a radiation dominated Universe, the Hubble parameter is given by \(H^2=8\pi ^{3}g_{\ast }T^4/(90M_{\rm pl}^3)\) 
and \(g_{\ast }\simeq 110\) .
The condition \(p(T)\sim 1\)  guarantees the percolation of bubbles in the early Universe and can be
translated into the following criterion for determining the nucleation temperature [1]}
\(\frac{S_3(T_{\rm n})}{T_{\rm n}}\simeq 4\ln \left( \frac{T_{\rm n}}{H} \right)\simeq 142-4\log \left( \frac{T_{\rm n}}{246~\rm GeV} \right).\) 
